The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
- Autores
- Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; Briceño, C.; Alexander, K. D.; Blanchard, P. K.; Chornock, R.; Cowperthwaite, P. S.; Eftekhari, T.; Fong, W.; Margutti, R.; Villar, V. A.; Williams, P. K. G.; Brown, W.; Annis, J.; Bahramian, A.; Brout, D.; Brown, D. A.; Chen, H. Y.; Clemens, J.C.; Dennihy, E.; Dunlap, B.; Holz, D.E.; Marchesini, Ezequiel Joaquín; Massaro, F.; Moskowitz, N.; Pelisoli, I.; Rest, A.; Ricci, F.; Sako, M.; Soares Santos, M.; Strader, J.
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis.
Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos
Fil: Metzger, B. D.. Columbia University In The City Of New York; Estados Unidos
Fil: Elias, J.. Southern Astrophysical Research Telescope; Chile
Fil: Briceño, C.. Cerro Tololo Inter American Observatory; Chile
Fil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Chornock, R.. Ohio University; Estados Unidos
Fil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Fong, W.. Northwestern University; Estados Unidos
Fil: Margutti, R.. Northwestern University; Estados Unidos
Fil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Annis, J.. Fermi National Accelerator Laboratory; Estados Unidos
Fil: Bahramian, A.. Michigan State University; Estados Unidos
Fil: Brout, D.. University of Pennsylvania; Estados Unidos
Fil: Brown, D. A.. Syracuse University; Estados Unidos
Fil: Chen, H. Y.. University of Chicago; Estados Unidos
Fil: Clemens, J.C.. University of North Carolina; Estados Unidos
Fil: Dennihy, E.. University of North Carolina; Estados Unidos
Fil: Dunlap, B.. University of North Carolina; Estados Unidos
Fil: Holz, D.E.. University of Chicago; Estados Unidos
Fil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; Argentina
Fil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; Italia
Fil: Moskowitz, N.. Lowell Observatory; Estados Unidos
Fil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino Unido
Fil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados Unidos
Fil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; Italia
Fil: Sako, M.. University of Pennsylvania; Estados Unidos
Fil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados Unidos
Fil: Strader, J.. Michigan State University; Estados Unidos - Materia
-
BINARIES: CLOSE
GRAVITATIONAL WAVES
NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES
STARS: NEUTRON - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/56893
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The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar EjectaNicholl, M.Berger, E.Kasen, D.Metzger, B. D.Elias, J.Briceño, C.Alexander, K. D.Blanchard, P. K.Chornock, R.Cowperthwaite, P. S.Eftekhari, T.Fong, W.Margutti, R.Villar, V. A.Williams, P. K. G.Brown, W.Annis, J.Bahramian, A.Brout, D.Brown, D. A.Chen, H. Y.Clemens, J.C.Dennihy, E.Dunlap, B.Holz, D.E.Marchesini, Ezequiel JoaquínMassaro, F.Moskowitz, N.Pelisoli, I.Rest, A.Ricci, F.Sako, M.Soares Santos, M.Strader, J.BINARIES: CLOSEGRAVITATIONAL WAVESNUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCESSTARS: NEUTRONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis.Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados UnidosFil: Metzger, B. D.. Columbia University In The City Of New York; Estados UnidosFil: Elias, J.. Southern Astrophysical Research Telescope; ChileFil: Briceño, C.. Cerro Tololo Inter American Observatory; ChileFil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Chornock, R.. Ohio University; Estados UnidosFil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Fong, W.. Northwestern University; Estados UnidosFil: Margutti, R.. Northwestern University; Estados UnidosFil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Annis, J.. Fermi National Accelerator Laboratory; Estados UnidosFil: Bahramian, A.. Michigan State University; Estados UnidosFil: Brout, D.. University of Pennsylvania; Estados UnidosFil: Brown, D. A.. Syracuse University; Estados UnidosFil: Chen, H. Y.. University of Chicago; Estados UnidosFil: Clemens, J.C.. University of North Carolina; Estados UnidosFil: Dennihy, E.. University of North Carolina; Estados UnidosFil: Dunlap, B.. University of North Carolina; Estados UnidosFil: Holz, D.E.. University of Chicago; Estados UnidosFil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; ArgentinaFil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; ItaliaFil: Moskowitz, N.. Lowell Observatory; Estados UnidosFil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino UnidoFil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados UnidosFil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; ItaliaFil: Sako, M.. University of Pennsylvania; Estados UnidosFil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados UnidosFil: Strader, J.. Michigan State University; Estados UnidosInstitute of Physics Publishing2017-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/56893Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-82041-8213CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/aa9029info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/2041-8213/aa9029/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:02:29Zoai:ri.conicet.gov.ar:11336/56893instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:02:29.681CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
title |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
spellingShingle |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta Nicholl, M. BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON |
title_short |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
title_full |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
title_fullStr |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
title_full_unstemmed |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
title_sort |
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta |
dc.creator.none.fl_str_mv |
Nicholl, M. Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J. |
author |
Nicholl, M. |
author_facet |
Nicholl, M. Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J. |
author_role |
author |
author2 |
Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J. |
author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
dc.subject.none.fl_str_mv |
BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON |
topic |
BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis. Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos Fil: Metzger, B. D.. Columbia University In The City Of New York; Estados Unidos Fil: Elias, J.. Southern Astrophysical Research Telescope; Chile Fil: Briceño, C.. Cerro Tololo Inter American Observatory; Chile Fil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Chornock, R.. Ohio University; Estados Unidos Fil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Fong, W.. Northwestern University; Estados Unidos Fil: Margutti, R.. Northwestern University; Estados Unidos Fil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Annis, J.. Fermi National Accelerator Laboratory; Estados Unidos Fil: Bahramian, A.. Michigan State University; Estados Unidos Fil: Brout, D.. University of Pennsylvania; Estados Unidos Fil: Brown, D. A.. Syracuse University; Estados Unidos Fil: Chen, H. Y.. University of Chicago; Estados Unidos Fil: Clemens, J.C.. University of North Carolina; Estados Unidos Fil: Dennihy, E.. University of North Carolina; Estados Unidos Fil: Dunlap, B.. University of North Carolina; Estados Unidos Fil: Holz, D.E.. University of Chicago; Estados Unidos Fil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; Argentina Fil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; Italia Fil: Moskowitz, N.. Lowell Observatory; Estados Unidos Fil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino Unido Fil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados Unidos Fil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; Italia Fil: Sako, M.. University of Pennsylvania; Estados Unidos Fil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados Unidos Fil: Strader, J.. Michigan State University; Estados Unidos |
description |
We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis. |
publishDate |
2017 |
dc.date.none.fl_str_mv |
2017-10 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/56893 Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-8 2041-8213 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/56893 |
identifier_str_mv |
Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-8 2041-8213 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/aa9029 info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/2041-8213/aa9029/meta |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Institute of Physics Publishing |
publisher.none.fl_str_mv |
Institute of Physics Publishing |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |